The complex stellar populations in the background of open clusters in the third Galactic quadrant
- Autores
- Carraro, Giovanni; Seleznev, Anton F.; Baume, Gustavo Luis; Turner, David G.
- Año de publicación
- 2016
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Multi-color photometry of the stellar populations in five fields in the third Galactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22, Ruprecht 11, and ESO489 SC01 is interpreted in terms of a warped and flared Galactic disk, without resort to an external entity such as the popular Monoceros or Canis Major overdensities. Except for NGC 2215, the clusters are poorly or unstudied previously. The data generate basic parameters for eachcluster, including the distribution of stars along the line of sight.We use star counts and photometric analysis, without recourse to Galactic-model-based predictions or interpretations, and confirms earlier results for NGC 2215 and NGC 2354. ESO489 SC01 is not a real cluster, while Haffner 22 is an overlooked cluster aged 2.5 Gyr. Conclusions for Ruprecht 11 are preliminary, evidence for a cluster being marginal. Fields surrounding the clusters show signaturesof young and intermediate-age stellar populations. The young population background to NGC 2354 and Ruprecht 11 lies 8?9 kpc from the Sun and 1 kpc below the formal Galactic plane, tracing a portion of the Norma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of the disk 1214 kpc from the Galactic center. The old population is metal poor with an age of 2 3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It has a large color spread and is difficult to locate precisely. Young and old populations followa pattern that depends critically on the vertical location of the thin and/or thick disk, and whether or not a particular line of sight intersects one, both, or none.
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Structure of galaxy
Galaxy disks
Galaxy
Open clusters
Associations (estrellas) - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/93734
Ver los metadatos del registro completo
id |
SEDICI_33f9fca365a24a3f866318483d195ce3 |
---|---|
oai_identifier_str |
oai:sedici.unlp.edu.ar:10915/93734 |
network_acronym_str |
SEDICI |
repository_id_str |
1329 |
network_name_str |
SEDICI (UNLP) |
spelling |
The complex stellar populations in the background of open clusters in the third Galactic quadrantCarraro, GiovanniSeleznev, Anton F.Baume, Gustavo LuisTurner, David G.Ciencias AstronómicasStructure of galaxyGalaxy disksGalaxyOpen clustersAssociations (estrellas)Multi-color photometry of the stellar populations in five fields in the third Galactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22, Ruprecht 11, and ESO489 SC01 is interpreted in terms of a warped and flared Galactic disk, without resort to an external entity such as the popular Monoceros or Canis Major overdensities. Except for NGC 2215, the clusters are poorly or unstudied previously. The data generate basic parameters for eachcluster, including the distribution of stars along the line of sight.We use star counts and photometric analysis, without recourse to Galactic-model-based predictions or interpretations, and confirms earlier results for NGC 2215 and NGC 2354. ESO489 SC01 is not a real cluster, while Haffner 22 is an overlooked cluster aged 2.5 Gyr. Conclusions for Ruprecht 11 are preliminary, evidence for a cluster being marginal. Fields surrounding the clusters show signaturesof young and intermediate-age stellar populations. The young population background to NGC 2354 and Ruprecht 11 lies 8?9 kpc from the Sun and 1 kpc below the formal Galactic plane, tracing a portion of the Norma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of the disk 1214 kpc from the Galactic center. The old population is metal poor with an age of 2 3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It has a large color spread and is difficult to locate precisely. Young and old populations followa pattern that depends critically on the vertical location of the thin and/or thick disk, and whether or not a particular line of sight intersects one, both, or none.Instituto de Astrofísica de La Plata2016-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf4031-4046http://sedici.unlp.edu.ar/handle/10915/93734enginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2016MNRAS.455.4031Cinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/455/4/4031/1276218?redirectedFrom=fulltextinfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2663info:eu-repo/semantics/altIdentifier/hdl/11336/35482info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:19:26Zoai:sedici.unlp.edu.ar:10915/93734Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:19:27.101SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
title |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
spellingShingle |
The complex stellar populations in the background of open clusters in the third Galactic quadrant Carraro, Giovanni Ciencias Astronómicas Structure of galaxy Galaxy disks Galaxy Open clusters Associations (estrellas) |
title_short |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
title_full |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
title_fullStr |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
title_full_unstemmed |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
title_sort |
The complex stellar populations in the background of open clusters in the third Galactic quadrant |
dc.creator.none.fl_str_mv |
Carraro, Giovanni Seleznev, Anton F. Baume, Gustavo Luis Turner, David G. |
author |
Carraro, Giovanni |
author_facet |
Carraro, Giovanni Seleznev, Anton F. Baume, Gustavo Luis Turner, David G. |
author_role |
author |
author2 |
Seleznev, Anton F. Baume, Gustavo Luis Turner, David G. |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Structure of galaxy Galaxy disks Galaxy Open clusters Associations (estrellas) |
topic |
Ciencias Astronómicas Structure of galaxy Galaxy disks Galaxy Open clusters Associations (estrellas) |
dc.description.none.fl_txt_mv |
Multi-color photometry of the stellar populations in five fields in the third Galactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22, Ruprecht 11, and ESO489 SC01 is interpreted in terms of a warped and flared Galactic disk, without resort to an external entity such as the popular Monoceros or Canis Major overdensities. Except for NGC 2215, the clusters are poorly or unstudied previously. The data generate basic parameters for eachcluster, including the distribution of stars along the line of sight.We use star counts and photometric analysis, without recourse to Galactic-model-based predictions or interpretations, and confirms earlier results for NGC 2215 and NGC 2354. ESO489 SC01 is not a real cluster, while Haffner 22 is an overlooked cluster aged 2.5 Gyr. Conclusions for Ruprecht 11 are preliminary, evidence for a cluster being marginal. Fields surrounding the clusters show signaturesof young and intermediate-age stellar populations. The young population background to NGC 2354 and Ruprecht 11 lies 8?9 kpc from the Sun and 1 kpc below the formal Galactic plane, tracing a portion of the Norma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of the disk 1214 kpc from the Galactic center. The old population is metal poor with an age of 2 3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It has a large color spread and is difficult to locate precisely. Young and old populations followa pattern that depends critically on the vertical location of the thin and/or thick disk, and whether or not a particular line of sight intersects one, both, or none. Instituto de Astrofísica de La Plata |
description |
Multi-color photometry of the stellar populations in five fields in the third Galactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22, Ruprecht 11, and ESO489 SC01 is interpreted in terms of a warped and flared Galactic disk, without resort to an external entity such as the popular Monoceros or Canis Major overdensities. Except for NGC 2215, the clusters are poorly or unstudied previously. The data generate basic parameters for eachcluster, including the distribution of stars along the line of sight.We use star counts and photometric analysis, without recourse to Galactic-model-based predictions or interpretations, and confirms earlier results for NGC 2215 and NGC 2354. ESO489 SC01 is not a real cluster, while Haffner 22 is an overlooked cluster aged 2.5 Gyr. Conclusions for Ruprecht 11 are preliminary, evidence for a cluster being marginal. Fields surrounding the clusters show signaturesof young and intermediate-age stellar populations. The young population background to NGC 2354 and Ruprecht 11 lies 8?9 kpc from the Sun and 1 kpc below the formal Galactic plane, tracing a portion of the Norma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of the disk 1214 kpc from the Galactic center. The old population is metal poor with an age of 2 3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It has a large color spread and is difficult to locate precisely. Young and old populations followa pattern that depends critically on the vertical location of the thin and/or thick disk, and whether or not a particular line of sight intersects one, both, or none. |
publishDate |
2016 |
dc.date.none.fl_str_mv |
2016-02 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
format |
article |
status_str |
publishedVersion |
dc.identifier.none.fl_str_mv |
http://sedici.unlp.edu.ar/handle/10915/93734 |
url |
http://sedici.unlp.edu.ar/handle/10915/93734 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2016MNRAS.455.4031C info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/455/4/4031/1276218?redirectedFrom=fulltext info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2663 info:eu-repo/semantics/altIdentifier/hdl/11336/35482 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
dc.format.none.fl_str_mv |
application/pdf 4031-4046 |
dc.source.none.fl_str_mv |
reponame:SEDICI (UNLP) instname:Universidad Nacional de La Plata instacron:UNLP |
reponame_str |
SEDICI (UNLP) |
collection |
SEDICI (UNLP) |
instname_str |
Universidad Nacional de La Plata |
instacron_str |
UNLP |
institution |
UNLP |
repository.name.fl_str_mv |
SEDICI (UNLP) - Universidad Nacional de La Plata |
repository.mail.fl_str_mv |
alira@sedici.unlp.edu.ar |
_version_ |
1844616068190961664 |
score |
13.070432 |